Radiative viscosity of neutron stars

Abstract

We study non-linear effects of radiative viscosity of $npe$ matter in neutron stars for both direct Urca process and modified Urca process, and find that non-linear effects will decrease the ratio of radiative viscosity to bulk viscosity from 1.5 to 0.5 (for direct Urca process) and 0.375 (for modified Urca process). Which means that for small oscillations of neutron star, the large fraction of oscillation energy is emitted as neutrinos; but for large enough ones, bulk viscous dissipation dominates.

11pages, 4 figures

References in corpus (5)

• Bulk viscosity of strange quark matter: Urca versus non-leptonic processes
• Bulk viscosity of spin-one color superconductors with two quark flavors
• Bulk viscosity in nuclear and quark matter: A short review
• Bulk viscosity of Mixed nucleon-hyperon-quark Matter in Neutron stars
• Dissipation of radial oscillations in compact stars

Cited by in corpus (4)

• Beta equilibrium under neutron star merger conditions
• Viscosity of neutron star matter and $r$-modes in rotating pulsars
• Mechanism of r-mode stability in young rapidly rotating pulsars
• The extension of radiative viscosity to superfluid matter